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	Dopasowanie SED	Synteza populacji gwiazdowych	Fotometria tranzytowa
Dziedzina	Astronomia	Astronomia	Astronomia
Rodzina	Process / pipeline	Process / pipeline	Process / pipeline
Rok powstania	2003	2003	1984
Twórca	Gustavo Bruzual	Gustavo Bruzual	William Borucki
Typ	Analysis and modeling method	Theoretical modeling method	Observational photometric pipeline
Źródło pierwotne	Bruzual, G., & Charlot, S. (2003). Stellar population synthesis at arbitrary metallicity with the Bruzual & Charlot models. Monthly Notices of the Royal Astronomical Society, 344(3), 1000-1028.	Bruzual, G., & Charlot, S. (2003). Stellar population synthesis at arbitrary metallicity with the Bruzual & Charlot models. Monthly Notices of the Royal Astronomical Society, 344(3), 1000-1028.	Borucki, W. J., & Summers, A. L. (1984). The photometric method of detecting other planetary systems. Astrophysical Journal, 281, 537-553.
Inne nazwy	SED Analysis, Spectral Energy Distribution Method, Photometric Redshift	SPS Models, Population Synthesis, Integrated Light Modeling	Photometric Transit Method, Planetary Transit Detection
Pokrewne	3	3	3
Podsumowanie	Spectral Energy Distribution (SED) fitting is the technique of comparing observed photometric measurements of galaxies across many wavelengths against theoretical predictions from stellar population synthesis models. By fitting models to observations, astronomers estimate galaxy properties including redshift, mass, age, star formation rate, and dust content without requiring expensive spectroscopic observations.	Stellar population synthesis is a technique for modeling the integrated light from a galaxy by summing the contributions of all individual stars formed at different times and with different masses and metallicities. Developed systematically by Bruzual and Charlot (2003), this approach enables estimation of fundamental galaxy properties from observations without detailed knowledge of individual stars.	Transit photometry is an observational technique that detects exoplanets by monitoring the periodic dips in stellar brightness as planets cross in front of their host stars. First systematized by William Borucki in 1984, this method became the most successful exoplanet detection technique, with the Kepler space telescope discovering thousands of confirmed exoplanets using this approach.